Discovery of the first young brown dwarf in the Serpens cluster

被引：16

作者：

Lodieu, N

Caux, E

Monin, JL

Klotz, A

机构：

[1] Astrophys Inst Potsdam, D-14482 Potsdam, Germany

[2] UPS, CNRS, CESR, F-31028 Toulouse 04, France

[3] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 09, France

[4] Inst Univ France, Paris, France

来源：

ASTRONOMY & ASTROPHYSICS | 2002年 / 383卷 / 03期

关键词：

stars : formation; stars : pre-main sequence; stars : low-mass; brown dwarfs; infrared : stars; techniques : photometric; techniques : spectroscopic;

D O I：

10.1051/0004-6361:20020034

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this letter, we report the discovery of the first young early L-dwarf in the Serpens cloud. It is obscured by more than ten magnitudes of visual absorption and was found during a near infrared (NIR) photometric survey of a 50 square arcmin area in the Serpens cloud, deep enough to probe the substellar domain. After selection from NIR colour-magnitude and colour-colour diagrams, its substellar nature has been confirmed by NIR spectroscopy at the VLT. We estimate the mass of this brown dwarf to be similar to0.05 M-. and its age to be similar to3.5 Myr. From its NIR indices, we estimate its present spectral type to be L0-L3, and using a model its future spectral type to be T. This is the first young brown dwarf ever found deeply embedded in a star formation region.

引用

页码：L15 / L18

页数：4

共 25 条

[1] The limiting effects of dust in brown dwarf model atmospheres [J].

Allard, F ;

Hauschildt, PH ;

Alexander, DR ;

Tamanai, A ;

Schweitzer, A .

ASTROPHYSICAL JOURNAL, 2001, 556 (01) :357-372

[2]

Baraffe I, 1998, ASTRON ASTROPHYS, V337, P403

[3] Observations of brown dwarfs [J].

Basri, G .

ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS, 2000, 38 :485-519

[4]

BEJAR VJS, 2001, IN PRESS APJ

[5]

Devillard N, 2001, ASTR SOC P, V238, P525

[6]

Devillard N, 1999, ASTR SOC P, V172, P333

[7]

EIROA C, 1992, ASTRON ASTROPHYS, V262, P468

[8]

GEBALLE TR, 2001, IN PRESS APJ

[9]

Giovannetti P, 1998, ASTRON ASTROPHYS, V330, P990

[10] K-band variability as a method to select young stellar object candidates [J].

Kaas, AA .

ASTRONOMICAL JOURNAL, 1999, 118 (01) :558-571

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